Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Hełminiak, K. G.; Konacki, Maciej

doi:10.1051/0004-6361/200913336

Cited by 24 publications

(10 citation statements)

References 72 publications

(57 reference statements)

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“…To date, only two other LMDEBs are known to be in a similar configuration: BD ‐22 5866, which is a system with a K7+K7 eclipsing pair and an M1+M2 non‐eclipsing binary (Shkolnik et al ), and YY Gem, which is the faintest member of a sextuple system, composed of three spectroscopic binaries, Castor A, B and C (α Gem ABC; Vinter Hansen, Neubauer & Roosen‐Raad ; Kron ; Bopp ). There are also a few examples of LMDEBs known to have a single additional companion, such as LP 133‐373 (Vaccaro et al ), HIP 96515 (Huélamo et al ), MR Del (Pribulla et al ; Djurašević et al ), NLTT 41135 (Irwin et al ), ASAS‐08 (Montes et al ; Hełminiak & Konacki ) or the triply eclipsing KOI‐126 (Carter et al ). Such systems not only allow more rigid constraints on the evolutionary models than in the cases of ‘lonely’ eclipsing binaries, but they also play an important role in testing star‐formation theories, stellar population codes and dynamical interactions in multiple stellar systems.…”

Section: Discussionmentioning

confidence: 99%

“…For the final orbital fit, we used all measurements simultaneously. We used the spectroscopic orbit fitting procedure described in our previous papers (Hełminiak et al ; Hełminiak & Konacki ; Hełminiak et al ). This simple code uses a Levenberg–Marquardt minimalization algorithm to find a Keplerian orbit of a spectroscopic binary.…”

Section: Spectroscopy and Radial Velocitiesmentioning

confidence: 99%

“…The eclipsing system ASAS J011328-3821.1 (2MASS J01132817-3821024, 1RXS J011328.8-382059, hereafter ASAS-01) has the shortest orbital period of all the objects in our sample of low-mass detached eclipsing binaries (LMDEBs; see: Hełminiak & Konacki 2011;Hełminiak et al 2011) found in the All-Sky Automated Survey (ASAS) Catalogue of Variable Stars (ACVS; Pojmański 2002), 1 and it is one of the shortest among the LMDEBs known to date (i.e. P ASAS = 0.44559 d).…”

Section: T H E a S A S J 0 1 1 3 8 -3 8 1 1 S Y S T E Mmentioning

confidence: 99%

“…The last spectrum was obtained in 2008 September with the 3.9-m AAT and its University College London Echelle Spectrograph (UCLES) at the Siding Spring Observatory, with the same settings as described in Hełminiak et al (2009Hełminiak et al ( , 2011. This spectrum was not binned, and after 900 s of exposure we reached S/N ratio ∼20 at λ = 6530 Å.…”

Section: Observationsmentioning

confidence: 99%

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Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

Hełminiak

Konacki

Rozyczka

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present the orbital and physical parameters of a newly discovered low‐mass detached eclipsing binary from the All‐Sky Automated Survey (ASAS) data base: ASAS J011328–3821.1 A, which is a member of a visual binary system with the secondary component separated by about 1.4 arcsec. The radial velocities have been calculated from the high‐resolution spectra obtained with the 1.9‐m Radcliffe telescope/Grating Instrument for Radiation Analysis with a Fibre‐Fed Echelle (GIRAFFE) spectrograph, the 3.9‐m Anglo‐Australian Telescope (AAT)/University College London Echelle Spectrograph (UCLES) and the 3.0‐m Shane telescope/Hamilton Spectrograph (HamSpec) on the basis of the todcor technique and the positions of the Hα emission lines. For the analysis, we have used V‐ and I‐band photometry obtained with the 1.0‐m Elizabeth telescope and the 0.41‐m Panchromatic Robotic Optical Monitoring and Polarimetry Telescopes (PROMPT), supplemented with the publicly available ASAS light curve of the system. We have found that ASAS J011328–3821.1 A is composed of two late‐type dwarfs, which have masses of M1 = 0.612 ± 0.030 M⊙ and M2 = 0.445 ± 0.019 M⊙ and radii of R1 = 0.596 ± 0.020 R⊙ and R2 = 0.445 ± 0.024 R⊙. Both show a substantial level of activity, which manifests in strong Hα and Hβ emission and the presence of cool spots. The influence of the third light on the eclipsing pair properties has also been evaluated and the photometric properties of component B have been derived. A comparison with several popular stellar evolution models shows that the system is on its main‐sequence evolution stage and that it is probably more metal‐rich than the Sun. We have also found several clues to suggest that component B itself is a binary composed of two nearly identical ∼0.5‐M⊙ stars.

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Section: Discussionmentioning

confidence: 99%

Section: Spectroscopy and Radial Velocitiesmentioning

confidence: 99%

Section: T H E a S A S J 0 1 1 3 8 -3 8 1 1 S Y S T E Mmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

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Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

Hełminiak

Konacki

Rozyczka

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Let us note that spots can easily induce RV variations at the level of a few hundreds of m s −1 so the RV variability of BY Dra is not surprising (see e.g. Hełminiak & Konacki 2011; Hełminiak et al 2011). We also had to adopt small shifts between each data set as is explained in Konacki et al (2010).…”

Section: Radial Velocitiesmentioning

confidence: 99%

New high-precision orbital and physical parameters of the double-lined low-mass spectroscopic binary BY Draconis

Hełminiak

Konacki

Muterspaugh

et al. 2011

Monthly Notices of the Royal Astronomical Society

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We present the most precise to date orbital and physical parameters of the well‐known short period (P= 5.975 d), eccentric (e= 0.3) double‐lined spectroscopic binary BY Draconis (BY Dra), a prototype of a class of late‐type, active, spotted flare stars. We calculate the full spectroscopic/astrometric orbital solution by combining our precise radial velocities (RVs) and the archival astrometric measurements from the Palomar Testbed Interferometer (PTI). The RVs were derived based on the high‐resolution echelle spectra taken between 2004 and 2008 with the Keck I/high‐resolution echelle spectrograph, Shane/CAT/HamSpec and TNG/SARG telescopes/spectrographs using our novel iodine‐cell technique for double‐lined binary stars. The RVs and available PTI astrometric data spanning over eight years allow us to reach 0.2–0.5 per cent level of precision in Msin 3i and the parallax but the geometry of the orbit (i≃ 154°) hampers the absolute mass precision to 3.3 per cent, which is still an order of magnitude better than for previous studies. We compare our results with a set of Yonsei–Yale theoretical stellar isochrones and conclude that BY Dra is probably a main‐sequence system more metal rich than the Sun. Using the orbital inclination and the available rotational velocities of the components, we also conclude that the rotational axes of the components are likely misaligned with the orbital angular momentum. Given BY Dra’s main‐sequence status, late spectral type and the relatively short orbital period, its high orbital eccentricity and probable spin–orbit misalignment are not in agreement with the tidal theory. This disagreement may possibly be explained by smaller rotational velocities of the components and the presence of a substellar mass companion to BY Dra AB.

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Weighing stars from birth to death: mass determination methods across the HRD

Serenelli

Weiß

Aerts

et al. 2021

Astron Astrophys Rev

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The mass of a star is the most fundamental parameter for its structure, evolution, and final fate. It is particularly important for any kind of stellar archaeology and characterization of exoplanets. There exist a variety of methods in astronomy to estimate or determine it. In this review we present a significant number of such methods, beginning with the most direct and model-independent approach using detached eclipsing binaries. We then move to more indirect and model-dependent methods, such as the quite commonly used isochrone or stellar track fitting. The arrival of quantitative asteroseismology has opened a completely new approach to determine stellar masses and to complement and improve the accuracy of other methods. We include methods for different evolutionary stages, from the pre-main sequence to evolved (super)giants and final remnants. For all methods uncertainties and restrictions will be discussed. We provide lists of altogether more than 200 benchmark stars with relative mass accuracies between ½0:3; 2% for the covered mass range of M 2 ½0:1; 16 M , 75% of which are stars burning hydrogen in their core and the other 25% covering all other evolved stages. We close with a recommendation how to combine various methods to arrive at a ''mass-ladder'' for stars.

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Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Cited by 24 publications

References 72 publications

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue - IV. A 0.61 + 0.45 M⊙ binary in a multiple system

New high-precision orbital and physical parameters of the double-lined low-mass spectroscopic binary BY Draconis

Weighing stars from birth to death: mass determination methods across the HRD

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